Impact of oxygen fugacity on the atmospheric structure and emission spectra of ultra-hot rocky exoplanets

Context. Atmospheres above lava-ocean planets (LOPs) hold clues related to the properties of their interiors, based on the expectation that the two reservoirs are in chemical equilibrium. Furthermore, such atmospheres are observable with current-generation space- and ground-based telescopes. While efforts have been made to understand how emission spectra are related to the composition of the lava ocean, the influence of oxygen fugacity has yet to be examined in a self-consistent way. Aims. Here, we investigate the sensitivity of atmospheric emission spectra of LOPs to key geochemical parameters, namely, temperature ( T ), composition ( X ), and oxygen fugacity ( f O 2 ). We also consider the precision involved in recovering these spectra from observations of hot, rocky exoplanets. Methods. We considered ‘mineral’ atmospheres produced in equilibrium with silicate liquids. We treated f O 2 as an independent variable, together with T and X , to compute equilibrium partial pressures ( p ) of stable gas species at the liquid-gas interface. Above this boundary, the atmospheric speciation and the pressure–temperature structure are computed self-consistently to yield emission spectra. We explored a wide array of plausible compositions, oxygen fugacities (between 6 log 10 units below and above the iron-wüstite buffer, IW), and irradiation temperatures (2000, 2500, 3000, and 3500 K) relevant to LOPs. Results. We find that SiO(g), Fe(g) and Mg(g) are the major species below ~IW, ceding to O 2 (g) and O(g) in more oxidised atmospheres. The transition between the two regimes demarcates a minimum in total pressure ( P ). Because p scales linearly with X , emission spectra are only modest functions of composition. By contrast, f O 2 can vary over orders of magnitude, thereby causing commensurate changes in p. Atmospheres outgassed from reducing melts exhibit intense SiO emission, creating a temperature inversion in the upper atmosphere. Conversely, oxidised atmospheres have lower p SiO and lack thermal inversions, with their resulting emission spectra mimicking that of a black-body. Consequently, the intensity of SiO emission relative to the background, generated by MgO(g), can be used to quantify the f O 2 of the atmosphere. Depending on the emission spectroscopy metric of the target, deriving the f O 2 of known nearby LOPs is possible with a few secondary occultations observed by JWST.